Uncorrelated velocity and size residuals across galaxy rotation curves

Abstract

The mass--velocity--size relation of late-type galaxies decouples into independent correlations between mass and velocity (the Tully-Fisher relation), and between mass and size. This behaviour is different to early-type galaxies which lie on a Fundamental Plane. We study the coupling of the Tully-Fisher and mass-size relations in observations (the SPARC sample) and in empirical galaxy formation models based on halo abundance matching, and rotation curve fits with a hydrodynamically motivated halo profile. We systematically investigate the correlation coefficient between the Tully-Fisher residuals $\Delta V_r$ and mass-size residuals $\Delta R$ as a function of the radius $r$ at which the velocity is measured, and thus present the $\Delta V_r-\Delta R$ relation across rotation curves. We find no significant correlation in either the data or models for any $r$, aside from $r\ll R_{\text{eff}}$ where baryonic mass dominates. We show that this implies an anticorrelation between galaxy size and halo concentration (or halo mass) at fixed baryonic mass, and provides evidence against the hypothesis that galaxy and halo specific angular momentum are proportional. Finally, we study the $\Delta V_r-\Delta R$ relations produced by the baryons and dark matter separately by fitting halo profiles to the rotation curves. The balance between these components illustrates the "disk-halo conspiracy" required for no overall correlation.

arXiv comment7 pages, 4 figures; revised to match MNRAS published version

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• The evolution of compact massive quiescent and starforming galaxies derived from the $R_e-R_h$ and $M_{\mathrm{star}}-M_h$ relations
• On the fundamentality of the radial acceleration relation for late-type galaxy dynamics
• Inferring dark matter halo properties for HI-selected galaxies
• The impact of the halo spin-concentration relation on disc scaling laws
• Bounding the Cosmological Constant using Galactic Rotation Curves from the SPARC Dataset
• Testing subhalo abundance matching with galaxy kinematics